Clumpy disc and bulge formation

Josefa Perez, Octavio Valenzuela, Patricia B. Tissera, Leo Michel-Dansac

Resultado de la investigación: Article

23 Citas (Scopus)

Resumen

We present a set of hydrodynamical/N-body controlled simulations of isolated gas-rich galaxies that self-consistently include supernova (SN) feedback and a detailed chemical evolution model, both tested in cosmological simulations. The initial conditions are motivated by the observed star-forming galaxies at z̃2-3.We find that the presence of a multiphase interstellar media in our models promotes the growth of disc instability favouring the formation of clumps which, in general, are not easily disrupted on time-scales compared to the migration time. We show that stellar clumps migrate towards the central region and contribute to form a classicallike bulge with a Séersic index, n>2. Our physically motivated SNfeedback has a mild influence on clump survival and evolution, partially limiting the mass growth of clumps as the energy released per SN event is increased, with the consequent flattening of the bulge profile. This regulation does not prevent the building of a classical-like bulge even for the most energetic feedback tested. Our SN feedback model is able to establish self-regulated star formation, producing mass-loaded outflows and stellar age spreads comparable to observations. We find that the bulge formation by clumps may coexist with other channels of bulge assembly such as bars and mergers. Our results suggest that galactic bulges could be interpreted as composite systems with structural components and stellar populations storing archaeological information of the dynamical history of their galaxy.

Idioma originalEnglish
Número de artículostt1563
Páginas (desde-hasta)259-265
Número de páginas7
PublicaciónMonthly Notices of the Royal Astronomical Society
Volumen436
N.º1
DOI
EstadoPublished - 1 nov 2013

Huella dactilar

clumps
supernovae
galaxies
structural component
merger
simulation
outflow
energetics
galactic bulge
chemical evolution
timescale
flattening
star formation
history
gas
assembly
energy
histories
stars
composite materials

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Perez, Josefa ; Valenzuela, Octavio ; Tissera, Patricia B. ; Michel-Dansac, Leo. / Clumpy disc and bulge formation. En: Monthly Notices of the Royal Astronomical Society. 2013 ; Vol. 436, N.º 1. pp. 259-265.
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abstract = "We present a set of hydrodynamical/N-body controlled simulations of isolated gas-rich galaxies that self-consistently include supernova (SN) feedback and a detailed chemical evolution model, both tested in cosmological simulations. The initial conditions are motivated by the observed star-forming galaxies at z̃2-3.We find that the presence of a multiphase interstellar media in our models promotes the growth of disc instability favouring the formation of clumps which, in general, are not easily disrupted on time-scales compared to the migration time. We show that stellar clumps migrate towards the central region and contribute to form a classicallike bulge with a S{\'e}ersic index, n>2. Our physically motivated SNfeedback has a mild influence on clump survival and evolution, partially limiting the mass growth of clumps as the energy released per SN event is increased, with the consequent flattening of the bulge profile. This regulation does not prevent the building of a classical-like bulge even for the most energetic feedback tested. Our SN feedback model is able to establish self-regulated star formation, producing mass-loaded outflows and stellar age spreads comparable to observations. We find that the bulge formation by clumps may coexist with other channels of bulge assembly such as bars and mergers. Our results suggest that galactic bulges could be interpreted as composite systems with structural components and stellar populations storing archaeological information of the dynamical history of their galaxy.",
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Perez, J, Valenzuela, O, Tissera, PB & Michel-Dansac, L 2013, 'Clumpy disc and bulge formation', Monthly Notices of the Royal Astronomical Society, vol. 436, n.º 1, stt1563, pp. 259-265. https://doi.org/10.1093/mnras/stt1563

Clumpy disc and bulge formation. / Perez, Josefa; Valenzuela, Octavio; Tissera, Patricia B.; Michel-Dansac, Leo.

En: Monthly Notices of the Royal Astronomical Society, Vol. 436, N.º 1, stt1563, 01.11.2013, p. 259-265.

Resultado de la investigación: Article

TY - JOUR

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AU - Perez, Josefa

AU - Valenzuela, Octavio

AU - Tissera, Patricia B.

AU - Michel-Dansac, Leo

PY - 2013/11/1

Y1 - 2013/11/1

N2 - We present a set of hydrodynamical/N-body controlled simulations of isolated gas-rich galaxies that self-consistently include supernova (SN) feedback and a detailed chemical evolution model, both tested in cosmological simulations. The initial conditions are motivated by the observed star-forming galaxies at z̃2-3.We find that the presence of a multiphase interstellar media in our models promotes the growth of disc instability favouring the formation of clumps which, in general, are not easily disrupted on time-scales compared to the migration time. We show that stellar clumps migrate towards the central region and contribute to form a classicallike bulge with a Séersic index, n>2. Our physically motivated SNfeedback has a mild influence on clump survival and evolution, partially limiting the mass growth of clumps as the energy released per SN event is increased, with the consequent flattening of the bulge profile. This regulation does not prevent the building of a classical-like bulge even for the most energetic feedback tested. Our SN feedback model is able to establish self-regulated star formation, producing mass-loaded outflows and stellar age spreads comparable to observations. We find that the bulge formation by clumps may coexist with other channels of bulge assembly such as bars and mergers. Our results suggest that galactic bulges could be interpreted as composite systems with structural components and stellar populations storing archaeological information of the dynamical history of their galaxy.

AB - We present a set of hydrodynamical/N-body controlled simulations of isolated gas-rich galaxies that self-consistently include supernova (SN) feedback and a detailed chemical evolution model, both tested in cosmological simulations. The initial conditions are motivated by the observed star-forming galaxies at z̃2-3.We find that the presence of a multiphase interstellar media in our models promotes the growth of disc instability favouring the formation of clumps which, in general, are not easily disrupted on time-scales compared to the migration time. We show that stellar clumps migrate towards the central region and contribute to form a classicallike bulge with a Séersic index, n>2. Our physically motivated SNfeedback has a mild influence on clump survival and evolution, partially limiting the mass growth of clumps as the energy released per SN event is increased, with the consequent flattening of the bulge profile. This regulation does not prevent the building of a classical-like bulge even for the most energetic feedback tested. Our SN feedback model is able to establish self-regulated star formation, producing mass-loaded outflows and stellar age spreads comparable to observations. We find that the bulge formation by clumps may coexist with other channels of bulge assembly such as bars and mergers. Our results suggest that galactic bulges could be interpreted as composite systems with structural components and stellar populations storing archaeological information of the dynamical history of their galaxy.

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KW - Galaxies: evolution

KW - Galaxies: formation Galaxies: interactions.

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